Modelling the Milky Way through adiabatic compression of cold dark matter haloes

V. F. Cardone; M. Sereno

doi:10.1051/0004-6361:20042035

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Volume 438 / No 2 (August I 2005)

A&A, 438 2 (2005) 545-556

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Issue		A&A Volume 438, Number 2, August I 2005


Page(s)		545 - 556
Section		Galactic structure, stellar clusters, and populations
DOI		https://doi.org/10.1051/0004-6361:20042035
Published online		08 July 2005

A&A 438, 545-556 (2005)

Modelling the Milky Way through adiabatic compression of cold dark matter haloes

V. F. Cardone¹ and M. Sereno²^,3

¹ Dipartimento di Fisica “E.R. Caianiello”, Università di Salerno, and INFN, Sez. di Napoli, Gruppo Coll. di Salerno, via S. Allende, 84081 Baronissi (Salerno), Italy e-mail: winny@na.infn.it
² Dipartimento di Scienze Fisiche, Università di Napoli, and INFN, Sez. di Napoli, Complesso Universitario di Monte S. Angelo, via Cinthia, 80126 Napoli, Italy
³ Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy

Received: 21 September 2004
Accepted: 19 January 2005

Abstract

We use the adiabatic compression theory to build a physically well-motivated Milky Way mass model in agreement with observational data. The visible mass of the Galaxy is distributed in a spheroidal bulge and a multi-component disc parametrized by three galactic parameters, the Sun distance to the galactic centre, R₀, the total bulge mass, $M_{{\rm bulge}}$ , and the local disc surface density, $\Sigma_{\odot}$ . To model the dark matter component, we adiabatically compress a Navarro, Frenk and White (NFW) halo (with concentration c and total mass $M_{{\rm vir}}$ ) for fixed values of the spin parameter λ, the fraction of the mass in baryons m_b, and the thin disc contribution to total angular momentum j_d. An iterative selection procedure is used to explore in detail the wide space of parameters only selecting those combinations of $\left\{ R_0, M_{{\rm bulge}}, \Sigma_{\odot}, \lambda, m_{\rm b}, j_{\rm d}, c, M_{{\rm vir}} \right\}$ that give rise to a Milky Way model in agreement with observational constraints. This analysis leads us to conclude that only models with $R_0 = 8.5$ kpc, $0.8 \times 10^{10}~M_{\odot} < M_{{\rm bulge}} < 1.6 \times 10^{10}~M_{\odot}$ and $49~M_{\odot}~{\rm pc}^{-2} \le \Sigma_{\odot} \le 56~M_{\odot}~{\rm pc}^{-2}$ can be reconciled with the set of observational constraints. As regards the parameters entering the adiabatic compression, we find $0.03 \le \lambda \le 0.10$ and $0.04 \le m_{\rm b} \le 0.10$ , while final estimates of the parameters describing the initial halo profile turn out to be $5 \la c \la 12$ and $7 \times 10^{11}~M_{\odot} \la M_{{\rm vir}} \la 17 \times 10^{11}~M_{\odot}$ (all at 95.7% CL).

Key words: Galaxy: kinematics and dynamics / Galaxy: structure / galaxies: formation / dark matter

© ESO, 2005

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